We report absolutely-calibrated photometry of the Saturnian
satellites in canonical near-infrared filters, including the
first such spectrum of the leading side of Enceladus. The
satellites were observed during Ring Plane Crossing in
August and September of 1995 with the NSFCAM instrument at
the NASA/IRTF. These observations were also simultaneous
with those of the Uranian system, taken with the same
instrument and filters, and analyzed by Baines {\it et al.}
({\it Icarus} {\bf 132}, 266-284, 1998). Results are
reported for J, H, and K filters near 1.27, 1.62, and 2.20
\mum, and two 0.1 \mum-wide filters centered at 1.73 and
2.27 \mum. We find that Enceladus has a peak brightness at
1.27 \mum with a geometric albedo of 0.898 ± 0.063, in
contrast to the Uranian satellites Miranda, Ariel, and
Titania, which are relatively dim at this wavelength
(albedos of roughly 0.3). The J-H band depth of Enceladus is
about 30%, characteristic of spectra of Rhea, Tethys, and
the trailing side of Iapetus, taken from Clark {\it et al.}
({\it Icarus} {\bf 58}, 265-281, 1984) and convolved with
our filters. By contrast, the darker Uranian satellites
display a J-H band depth of less than 10%. From H to 1.73
\mum, the full-disk albedo of Enceladus increases by 27%,
similar to the Uranian satellites. The dip in the Enceladus
spectrum from J to H, as well as the subsequent rise from H
to 1.73 \mum, are an expected signature of water ice.
Finally, preliminary results for the albedos of Tethys,
Dione, Rhea, and Mimas, as well as Enceladus, at 2.27 \mum
compare favorably with the visible albedos of Buratti and
Veverka ({\it Icarus}, {\bf 58}, 254-264, 1984).